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The broadening of metallic lines in cool stars

Published online by Cambridge University Press:  25 May 2016

S. D. Anstee ,
B. J. O'Mara  and
J. E. Ross
S. D. Anstee
Affiliation:
The University of Queensland, St. Lucia Queensland 4072, Australia
B. J. O'Mara
Affiliation:
The University of Queensland, St. Lucia Queensland 4072, Australia
J. E. Ross
Affiliation:
The University of Queensland, St. Lucia Queensland 4072, Australia

Abstract

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A theory for the broadening of spectral lines by collisions with atomic hydrogen developed by Anstee and O'Mara [1] is described and when applied to strong lines of elements in the sun leads to abundances which are independent of non-thermal motions in the photosphere and in excellent agreement with meteoritic values. In the case of the solar abundance of iron the results lead to a resolution of recent conflict concerning possible differences between the abundance of iron in the sun and meteorites. Excellent results obtained with the Mg b-lines permit these lines to be used in abundance determinations in other stars and also makes them particularly useful in determining the temperature structure in cool stars.

Type
Stellar Abundances
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 179 - 183
Copyright
Copyright © Kluwer 1997 

References

1. Anstee, S. D. and O'Mara, B. J. MNRAS , 253(4A):549, 1991.CrossRefGoogle Scholar
2. Anstee, S. D. and O'Mara, B. J. MNRAS , 276:859, 1995.CrossRefGoogle Scholar
3. Anstee, S. D., O'Mara, B. J., and Ross, J. E. MNRAS , 284:202, 1997.CrossRefGoogle Scholar
4. Ross, J. E. Spectrum synthesis program. http://www.uq.edu.au/~phjross/syn.htm.Google Scholar
5. Holweger, H. and Müller, E. A. Solar Phys. , 39:19, 1974.CrossRefGoogle Scholar
6. Carter, W. W. Phys. Rev. , 76:962, 1949.CrossRefGoogle Scholar